A two dimensional model for the chromosphere and the corona based on the idea that the magnetic flux is strongly concentrated at the boundaries of supergranule convection cells has been proposed by Gabriel in 1976. Thus he introduced a non-trivial geometry, the so-called ``funnel'', which is defined by the magnetic field lines. Dowdy et al. (1987) investigated the influence of the shape of the funnel on the temperature profile, i.e. on the ability to heat the corona. Since the magnetic field lines of the funnel are open field lines, the plasma is free to move along this field lines and eventually builds up the solar wind. In both of the aforementioned models this effect has been neglected. Based on a two dimensional funnel model we investigate the plasma flow. Also heat conduction, radiative losses and a heating function are considered. We linked our model to the observed quantities at the transition region and the lower solar corona at ~15000 km above the photosphere. The thereby found height profiles of the plasma properties within the funnel are presented.
CESRA Workshop on Coronal Explosive Events
- Pub Date: